The supporting measurements of the 'activity indicators' such as the FWHM and BIS of CCF and the Ca II H and K values from HARPS allow us to examine the intrinsic stellar variability. [1]} suggests that one can check two simple characteristics to look for changes in the shape of CCF: the width parameter FWHM and its BIS, computed following [2]}. The chromospheric activity is typically quantified by the S-index, as noted by [3]}. The S-index varies linearly with the chromospheric emission flux in the cores of the Ca II H and K lines in the near ultraviolet [4]}. From both panels of the Figure  REF , the mean value for S-index can be calculated as 0.3569 in the 2008-9 season and 0.2759 in 2012 and is denoted by the grey horizontal dashed line. The lower mean value in 2012 indicates that the star was less active during 2012.
